The vast thin plane of M31 corotating dwarfs: an additional fossil signature of the M31 merger and of its considerable impact in the whole Local Group
The vast thin plane of M31 corotating dwarfs: an additional fossil signature of the M31 merger and of its considerable impact in the whole Local Group
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M31 共转矮星的巨大薄平面：M31 合并及其对整个本地群的巨大影响的附加化石特征
DOI：
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发表时间：
2013
期刊：
影响因子：
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通讯作者：
H Germany
中科院分区：
文献类型：
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作者：
F. Hammer;Yanbin Yang;S. Fouquet;M. Pawlowski;P. Kroupa;M. Puech;H. Flores;Jianling Wang Laboratoire Gepi;O. Paris;France National Astronomical Observatoires;Chinese Academy of Sciences;C. I. F. Astronomy;U. Bonn;Bonn;H Germany
Ibata等人（2013）最近发现M31周围有一个巨大的薄卫星盘（VTDS），这对理解本星系群的性质提出了新的挑战。这是除了麦哲伦云（MC）意外接近银河系（MW）和另一个巨大的极地结构（VPOS），这几乎是垂直于我们的银河系盘。我们发现VTDS平面与M31外围的几个恒星潮汐流相重合，其速度分布与巨星流（GS）的速度分布一致。这暗示了一种共同的物理机制，可能与合并潮汐相互作用有关，知道类似的论点可能适用于MW位置的VPOS。此外，VTDS指向MW，与VPOS一样几乎垂直于MW盘。我们比较这些属性的建模M31作为一个古老的，富含气体的主要合并，已成功地用于预测M31子结构和GS的起源。我们发现，没有NE调谐，诱导的潮汐尾巴躺在VTDS平面，提供了一个单一的和共同的起源，许多恒星流和巨大的恒星结构周围的MW和M31。该模型还相当准确地再现VTDS dSphs的位置和速度。我们的推测导致了对本星系群过去历史的一种新的解释，因为由于M31古老的合并而产生的巨大的潮汐尾预计将向MW发送物质，包括MC。M31和MW之间的这种联系预计是非常特殊的，尽管它可能与附近星系中MW-MCs系统的稀有性报告定性一致。
The recent discovery by Ibata et al. (2013) of a vast thin disk of satellites (VTDS) around M31 oers a new challenge for the understanding of the Local Group properties. This comes in addition to the unexpected proximity of the Magellanic Clouds (MCs) to the Milky Way (MW), and to another vast polar structure (VPOS), which is almost perpendicular to our Galaxy disk. We nd that the VTDS plane is coinciding with several stellar, tidally-induced streams in the outskirts of M31, and, that its velocity distribution is consistent with that of the Giant Stream (GS). This is suggestive of a common physical mechanism, likely linked to merger tidal interactions, knowing that a similar argument may apply to the VPOS at the MW location. Furthermore, the VTDS is pointing towards the MW, being almost perpendicular to the MW disk, as the VPOS is. We compare these properties to the modelling of M31 as an ancient, gas-rich major merger, which has been successfully used to predict the M31 substructures and the GS origin. We nd that without ne tuning, the induced tidal tails are lying in the VTDS plane, providing a single and common origin for many stellar streams and for the vast stellar structures surrounding both the MW and M31. The model also reproduces quite accurately positions and velocities of the VTDS dSphs. Our conjecture leads to a novel interpretation of the Local Group past history, as a gigantic tidal tail due to the M31 ancient merger is expected to send material towards the MW, including the MCs. Such a link between M31 and the MW is expected to be quite exceptional, though it may be in qualitative agreement with the reported rareness of MW-MCs systems in nearby galaxies.
影响因子：
6.5
作者：
C. Foster;A. Hopkins;M. Gunawardhana;M. Lara-López;R. Sharp;O. Steele;E. Taylor;S. Driver;I. K. Baldryi;S. Bamford;J. Liske;J. Loveday;P. Norberg;J. Peacock;M. Alpaslan;A. Bauer;J. Bland-Hawthorn;S. Brough;E. Cameron;M. Colless;C. Conselice;S. Croom;C. Frenk;D. Hill;D. Jones;L. Kelvin;K. Kuijken;R. Nichol;M. Owers;H. Parkinson;K. Pimbblet;C. Popescu;M. Prescott;A. Robotham;Á. López-Sánchez;W. Sutherland;D. Thomas;R. Tuffs;E. V. Kampen;D. Wijesinghe
通讯作者：
C. Foster;A. Hopkins;M. Gunawardhana;M. Lara-López;R. Sharp;O. Steele;E. Taylor;S. Driver;I. K. Baldryi;S. Bamford;J. Liske;J. Loveday;P. Norberg;J. Peacock;M. Alpaslan;A. Bauer;J. Bland-Hawthorn;S. Brough;E. Cameron;M. Colless;C. Conselice;S. Croom;C. Frenk;D. Hill;D. Jones;L. Kelvin;K. Kuijken;R. Nichol;M. Owers;H. Parkinson;K. Pimbblet;C. Popescu;M. Prescott;A. Robotham;Á. López-Sánchez;W. Sutherland;D. Thomas;R. Tuffs;E. V. Kampen;D. Wijesinghe